Impact of the disk magnetization on MHD disk wind signature

Abstract

Observation of blue-shifted X-ray absorption lines indicates the presence of wind from the accretion disk in X-ray binaries. Magnetohydrodynamic (MHD) driving is one of the possible wind launching mechanisms. Recent theoretical development makes magnetic accretion-ejection self-similar solutions much more generalized, and wind can be launched even at much lower magnetization compared to equipartition value, which was the only possibility beforehand. Here, we model the transmitted spectra through MHD driven photoionized wind - models which have different values of magnetizations. We investigate the possibility of detecting absorption lines by the upcoming instruments XRISM and Athena. Attempts are made to find the robustness of the method of fitting asymmetric line profiles by multiple Gaussians. We use photoionization code XSTAR to simulate the transmitted model spectra. Fake observed spectra are finally produced by convolving model spectra with instruments' responses. Since the line asymmetries are apparent in the convolved spectra as well, this can be used as an observable diagnostic to fit for, in future XRISM and Athena spectra. We demonstrate some amount of rigor in assessing the equivalent widths of the major absorption lines, including the Fe XXVI Ly$\alpha$ doublets which can be clearly distinguished in the superior quality, future high resolution spectra. Disk magnetization becomes another crucial MHD variable that can significantly alter the absorption line profiles. Low magnetization pure MHD outflow models are dense enough to be observed by the existing or upcoming instruments. Thus these models become simpler alternatives to MHD-thermal models. Fitting with multiple Gaussians is a promising method to handle asymmetric line profiles, as well as the Fe XXVI Ly$\alpha$ doublets.

17 pages (including 4 pages of Appendix), 13 figures, Accepted for publication in A&A

References in corpus (24)

• X-ray Properties of Black-Hole Binaries
• Modelling the behaviour of accretion flows in X-ray binaries
• The magnetic nature of disk accretion onto black holes
• The Accretion Disk Wind in the Black Hole GRO J1655-40
• Spectrum Synthesis Modeling of the X-ray Spectrum of GRO J1655-40 Taken During the 2005 Outburst
• Hard-state accretion disk winds from black holes: the revealing case of MAXI J1820+070
• The role of the disk magnetization on the hysteresis behavior of X-ray binaries
• Magnetically-driven jets and winds from weakly magnetized accretion disks
• A unified accretion-ejection paradigm for black hole X-ray binaries. IV. Replication of the 2010--2011 activity cycle of GX 339-4
• Thermal Disk Winds in X-ray Binaries: Realistic Heating and Cooling Rates Give Rise to Slow, but Massive Outflows
• On the importance of special relativistic effects in modelling ultra-fast outflows
• Hard-state optical wind during the discovery outburst of the black-hole X-ray dipper MAXI J1803-298
• Optical and near-infrared spectroscopy of the black hole GX 339-4 II. The spectrocopic content in the low/hard and high/soft states
• Thermally-Driven Disc Winds as a Mechanism for X-ray Irradiation Heating in Black Hole X-ray Binaries: The Case Study of GX339-4
• A Comprehensive Chandra Study of the Disk Wind in the Black Hole Candidate 4U 1630-472
• Photoionization instability of the Fe K absorbing plasma in the neutron star transient AX J1745.6-2901
• Discovery of optical outflows and inflows in the black hole candidate GRS 1716-249
• Tell-Tale Spectral Signatures of MHD-driven Ultra-Fast Outflows in AGNs
• The current state of disk wind observations in BHLMXBs through X-ray absorption lines in the iron band
• Modeling Magnetic Disk-Wind State Transitions in Black Hole X-ray Binaries
• Simultaneous X-ray and optical spectroscopy of V404 Cygni supports the multi-phase nature of X-ray binary accretion disc winds
• Absorption lines from magnetically driven winds in X-ray binaries II: high resolution observational signatures expected from future X-ray observatories
• Numerical simulations of MHD jets from Keplerian accretion disks I-Recollimation shocks
• Hyper-massive Black Holes have Faint Broad and Narrow Emission Lines

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